Speaker
Description
We present a general-relativistic study of strongly magnetized neutron stars (NSs), using the XNS code to solve the coupled Einstein–Maxwell equations, focusing on (i) examining equilibrium configurations with both toroidal and poloidal magnetic field geometries, (ii) incorporating complex many-body effects through microscopically derived pairing gaps for proton superconductor, and (iii) employing equations of state (EoSs) derived from microscopic nuclear many-body theory with realistic two- and three-body forces, as well as from relativistic mean-field models. Across these EoSs, we compare superconducting topologies and analyze the influence of magnetic field geometry in models parameterized by central density. We further compute m ellipticities for several millisecond pulsars (MSPs), estimating their continuous gravitational-wave (CGW) emission. Although the predicted strains lie below the sensitivity of current detectors, next-generation observatories such as the Einstein Telescope and Cosmic Explorer may be able to detect these signals, providing an observational probe of superconductivity, magnetic field structure, and dense-matter microphysics in neutron stars.
